To be specific, we consider generation of gravitational waves by two compact
stars with equal masses \(m\)  moving along circular orbits of diameter \(r\) 
with angular velocity \(\Omega \)  (see Fig. REF ). \(\theta (t)=\Omega t+\theta _{0}\)  is the star azimuthal angle in the orbital plane.
Using formulas of Ref. [1]} we obtain that far from the binary
system
\(\mathbf {h}=-\frac{2Gm\Omega ^{2}r^{2}}{c^{4}R}\text{Re}\left[ \mathbf {P}e^{2i\theta (t)}\right] , \) 
